To consistently explain the observed broad-band spectrum, two-component models such as TBabs\(\times \) (diskbb+nthComp), TBabs\(\times \) (diskbb+powerlaw) and TBabs\(\times \) (nthComp+powerlaw) were further fitted to the data. The observed spectrum at both epochs (E1 & E2) were found to be reasonably well described by the TBabs\(\times \) (diskbb+nthComp) model, i.e, the combination of multi-colored disk blackbody component [1]}, [2]} and a thermal Comptonization model [3]}, [4]} modulated by Galactic absorption by neutral hydrogen [5]}. We found excesses around 1.3, 6.4 and 30 keV as shown in Fig. REF . An excess around 6.4 keV is indicative of an Fe emission line from the accretion disk, while the observed residuals around 30 keV indicate a Compton hump, which, together with the relativistically broadened Fe K\(\alpha \)  line, is typical for Compton reflection. A soft excess around 1.3 keV is typically observed when the surface of the accretion disk is ionized. In this case, electron scattering becomes important along with the re-emission of emission lines, causing a soft excess [6]}, [7]}, [8]}. We found that the red wing of the Fe emission line is extended down to 6 keV while the blue wing is stretched close to 8 keV with a dip around 11 keV as shown in Fig. REF .
